New Insights Into the Hydrologic History of Western Valles Marineris, Mars
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EPSC Abstracts Vol. 8, EPSC2013-281, 2013 European Planetary Science Congress 2013 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2013 New insights into the hydrologic history of western Valles Marineris, Mars J. Alexis P. Rodriguez (1) and V. C. Gulick (2) (1) NASA ARC/NPP, (2) NASA ARC/SETI Institute, NASA Ames Research Center, Mail Stop 239-20, Moffett Field, Ca, 94035 ([email protected] / Telephone: +1-604-07-74) Abstract 1b). However, its eastern and most distal parts exhibit a well-preserved lobate morphology (Fig. 2a). Using Mars Reconnaissance Orbiter (MRO) Context Examination of decameter-scale surface features (CTX) and High Resolution Imaging Science reveals an extensive system of polygonal fractures Experiment (HiRISE) image data in tandem with (Fig. 2b), coarsely layered-boundary outcrops (Fig. Mars Orbiter Laser Altimeter (MOLA) surface 2c), and channeled surfaces (Fig. 2d). Our topography, we have characterized and mapped the preliminary crater counts of this deposit indicate remnants of an extensive flow feature that we emplacement during the Early Hesperian, but this interpret to be a debris flow within the floors of result needs to be confirmed. Tithonium Chasma and an adjacent canyon system in western Valles Marineris. The deposit appears highly modified by collapse and tectonic deformation consistent with a freezing and devolatization history, but shows no signs of resurfacing by catastrophic floods. Preliminary impact crater count statistics indicate the deposit was emplaced during the Early Hesperian, thereby defining a stratigraphic marker that constrains any major surface water discharges from Noctis Labyrinthus to the Noachian period. 1. Introduction Noctis Labyrinthus and Valles Marineris form a vast network of canyons, ~4000 km in length, which are mostly (but not always) interconnected [1,2] (Fig. 1a). Ground-water circulation from aquifers located in the Tharsis Montes to Valles Marineris via Noctis Labyrinthus [3-5] may have led to development of the aquifers further east in circum-Chryse, which underwent collapse to form extensive outflow channels and chaotic terrains [3]. 2. Geomorphologic analysis Tithonium Chasma (Fig. 1b) comprises the largest undivided canyon in western Valles Marineris (Fig. 1a). We have identified an extensive sedimentary deposit that covers most of the chasma’s surface, and terminates within two canyons in western Valles Marineris (Fig. 1b). The eastern part of the deposit is extensively modified and exhibits morphology suggestive of surface collapse and fracturing (Fig. Figure 1: (a) MOLA context and location for the Figure 2: (a) CTX mosaic showing a perspective study region. (b) Map showing the eastern margins of view of lobated flow front within a canyon. (b, c and the flow deposit. d show HiRISE views of the deposit). (b) Scarp that exhibits coarse layering and matrix supported boulders. (b) Part of fractured surface. (c) Part of channeled surface, including localized meanders and bouldery deposits exposed within inverted channels. 3. Interpretations Our findings indicate that during the Early Hesperian, large volumes of water-saturated sediments were discharged from Noctis Labyrinthus. The polygonal fractures are indicative of extensively tectonic resurfacing, perhaps consequential of freezing and d expansion, and/or volume loss and subsidence. The outcrops are layered and approximately horizontal suggesting that the debris flow velocities were not turbulent, however these could have been emplaced by magmatic or sedimentary volcanism eruptions within the deposit. The channels are indicative a ground-water release history and the inverted channels show that outstripping of surficial layers has been modest flowing fluvial activity. We see no evidence for a history of major catastrophic flooding or debris flow from this region following emplacement of the mapped deposit. Acknowledgements This research was supported by funds from the NASA NPP program and NASA’s MRO HiRISE. References [1] Masursky, H. et al.: Geologic map of the Phoenicis Lacus quadrangle of Mars, The Survey, Reston, Va., 1978. [2] Scott, D. H. and Tanaka, K. L.: Geologic map of the western equatorial region of Mars, U.S. Geol. Surv. Misc. Invest. Ser., pp. Map I-1802-A, 1986. [3] Hanna, J. C. and Phillips, R. J.: Hydrological modeling of the Martian crust with application to the pressurization of aquifers, J. Geophys. Res., 110, 2005. [4] Harrison, K. P. and Grimm, R. E.: Regionally compartmented groundwater flow on Mars, J. Geophys. Res., 114, E04004, 2009. [5] Montgomery, D. R. et al.: Continental-scale salt tectonics on Mars and the origin of Valles Marineris and associated outflow channels, Geological Society of America Bulletin, 121, 117-133, 2009. .